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Pulsar Wind Nebulae: the VHE – X-Ray Connection

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Pulsar Wind Nebulae: the VHE – X-Ray Connection Gerd Pühlhofer, Landessternwarte Heidelberg + IAAT Tübingen Pulsar wind nebulae: The VHE – X-ray connection HESS = High Energy Stereoscopic System Photo: © Philippe Plailly H.E.S.S.:H.E.S.S.: HighHigh EnergyEnergy StereoscopicStereoscopic SystemSystem H.E.S.S. collaboration: MPI für Kernphysik, Heidelberg Humboldt Univ. Berlin Ruhr-Univ. Bochum Univ. Hamburg Landessternwarte Heidelberg LLR, Ecole Polytechnique, Palaiseau LPNHE, Univ. de Paris VI-VII PCC, College de France, Paris Observatoire Paris-Meudon, LUTH CEA Saclay Univ. de Grenoble Univ. Monpellier II CESR Toulouse Durham Univ. University of Leeds Dublin Inst. for Adv. Studies Nicolaus Kopernikus Astr. Center, Warsaw Jagiellonian University, Cracow Institute of Nuclear Physics, Warsaw Four twelve meter optical dishes Space research center, Warsaw Charles Univ., Prag Khomas Highlands (Namibia) Yerewan Physics Inst. North-West Univ., Potchefstroom 1800 above sea level Univ. of Namibia, Windhoek Start of full operation end of 2003 Univ. Tübingen H.E.S.S. event reconstruction parameters: • Primary direction: < 0.1° • Field of view: 3° FWHM • Shower core: 10m → Energy resolution: 15% • Energy range: 0.1–100 TeV Cherenkov light from shower particles Photo: © Philippe Plailly THE VHE (>100 GeV) Galactic plane from the HESS GP survey THE VHE (>100 GeV) Galactic plane from the HESS GP survey Let’s blank out: • SNR shells: RXJ 1713-3946, Vela Jr, RCW 86 • Binaries: LS 5039, PSR B1259-63 • Stellar cluster association: HESS J1023-575 (Westerlund 2) • Molecular cloud associations (confirmed and likely): Galactic ridge, HESS J1745-303, HESS J1800-240 (W28 A), HESS J1834-087 (W41) • For several of the remaining sources, a pulsar wind nebula (PWN) identification is certain • For the vast majority of the rest, a PWN scenario is at least possible OverviewOverview • Some general statements about the relation between X-ray and VHE pulsar wind nebulae • Young vs. middle-aged and relic PWN • Pevatrons and INTEGRAL • Identification problem of large-offset VHE PWN • Underluminous X-ray PWN and associated issues Warning: totally biased towards VHE-detected PWN GeometryGeometry ofof aa pulsarpulsar windwind (nebula)(nebula) Sketch by Slane Neutron star Cold, non-emitting flow Acceleration of particles at termination shock Visible (i.e. emitting) pulsar wind nebula Possibly interaction with surrounding SNR (e.g. reverse shock) XX--rayray emittingemitting PWN:PWN: samplesample studystudy Chandra PWN review, Kargaltsev & Pavlov, astro-ph/0801.2602 XX--rayray emittingemitting PWN:PWN: samplesample studystudy ε or η: Efficiency of current pulsar energy loss into given observation band Large scatter of X-ray synchrotron efficiencies But fairly good correlation between nonthermal magnetospheric and PWN emission Chandra PWN review, Kargaltsev & Pavlov, astro-ph/0801.2602 “Usual”“Usual” XX--rayray PWNPWN seenseen withwith ChandraChandra Tori Bow shocks and wakes ''Mouse'' Gaensler et al. 2004 Tori and bow shocks/tails reflect pulsar geometry resp. motion This is not what will be dealt with in this talk Gaensler et al., 2006 IC 443 Ng & Romani 2003 PWN:PWN: thethe largestlargest identifiedidentified GalacticGalactic VHEVHE populationpopulation Several firmly HESS HESS identified VHE pulsar wind Nebulae (PWN) Many VHE PWN candidates Why identified: • known pulsar • morphology HESS HESS matches with X- ray PWN Most VHE PWN are •extended • displaced from the pulsar CosmicCosmic microwavemicrowave backgroundbackground …… … serves as homogeneous target for Inverse compton scattering of electrons WMAP Ka Credit: WMAP Science Team CMBCMB ++ GalacticGalactic “foreground”“foreground” In addition, stellar and dust radiation fields can boost IC emission Credit: WMAP Science Team WMAP Ka (Thermal and nonthermal) Stellar and dust photon fields are hard to access (esp. 3-D) TheThe youngyoung CrabCrab NebulaNebula (1000(1000 years)years) HEGRA collaboration, ApJ 2004, 614, 897 (Northern Hemisphere source) synchrotron branch IC branch compact source, high B-field (160 µG) → • high synchrotron efficiency, IC emission comparatively low • synchrotron photons produce relevant target field for IC (“SSC”) → IC coupled to B-field again TheThe youngyoung CrabCrab NebulaNebula (1000(1000 years)years) HEGRA collaboration, ApJ 2004, 614, 897 MeV TeV IC branch TheThe youngyoung CrabCrab NebulaNebula (1000(1000 years)years) HEGRA collaboration, ApJ 2004, 614, 897 MeV +IC from stellar fields TeV IC branch Extended pulsar wind nebulae from middle-aged pulsars • are simpler because IC scattering off external, in principle well known target photon fields • are much more common… FFX // FFVHE …… … or FVHE / FX: a widely used diagnostic tool useful for investigating VHE – X-ray source associations from Kargaltsev et al., ApJ 670, 2007 LifetimeLifetime ofof VHEVHE--emittingemitting electronselectrons from Aharonian et al., A&A 460, 2006 τ ≈ × 5 -3 -1 -1 VHE 3.1 10 (wr/eV cm ) (E/1 TeV) years η -3 2 wr = wph + 0.025 eV cm (B/µG) η normalisation factor due to KN suppression Wph energy density in photon fields (CMB, IR, starlight) → For low B-fields, the lifetime of VHE-emitting electrons can greatly exceed the lifetime of the X-ray - synchrotron emitting (higher-energy) electrons → The VHE PWN reflects the injection evolution of the pulsar HESSHESS J1640J1640--465:465: aa “relic”“relic” PWNPWN scenarioscenario MOST XMM-Newton Funk, Hinton, GP, et al., ApJ 662, 2007 G21.5G21.5--0.9,0.9, KesKes 75:75: CrabCrab companions?companions? G21.5-0.9 Edot = 3.3 × 1037 erg s-1 Kes 75 Chandra Chandra t ~ 1000 years (« tc) Camilo et al., ApJ 637, 2006 Edot = 8 × 1036 erg s-1 ≈ t ~ 800 years ( tc) Magnetar-like behaviour Gotthelf et al., ApJ 542, 2000 Credit: NASA/CXC/GSFC Credit: NASA/CXC/Manithoba/ Gavriil et al. Matheson & Safi-Harb Ng et al., astro-ph/0804.3384 HESS coll., Djannati-Atai et al. astro-ph/0710.2247 FX / FVHE ~ 30 → B ~ 15µG FX / FVHE ~ 10 → B ~ 10µG HESS: unresolved HESS: unresolved Below equipartition B-fields Vela-X: a middle-aged PWN Vela-X: a middle-aged PWN 1 ’ ROSAT contours: extended X-ray synchrotron(?) nebula Chandra: compact X-ray nebula VHE spectrum (peak!) interpreted as IC scattering 1 → × 45 ° Enonth ~ 2 10 erg Caveat: → this isn‘t the entire PWN (as seen in radio) Color map: H.E.S.S.: → sensitivity limited? VHE IC nebula VHEVHE ++ XX--raysrays inin casecase ofof aa hadronichadronic sourcesource Energy X-rays TeV flux electron synchrotron ~B² electron IC ~ ph.-field E2 dn/dE proton:π0 IC high B field (>10 µG) ~ B-2 Photon energy VelaVela X:X: nucleonicnucleonic PWN?PWN? Vela Jr. (HESS) Vela X (HESS) Hadronic model Horns et al, A&A 451, 2006 Leptonic model, e.g. de Jager et al., astro-ph/0803.0116 • Debate still somewhat open • Some criticism on the hadronic scenario • In this talk, the standard view of leptonically-dominated PWN is adopted • (hadronically mediated acceleration) “Relic”“Relic” pulsarpulsar windwind nebulaenebulae HESS J1825-137: Identification with X-ray PWN G 18.0-0.7 XMM-Newton Gaensler et al., ApJ 2003 Aharonian et al. (HESS coll.) A&A 460, 2006 ArchetypeArchetype forfor aa TeVTeV –– XX--rayray PWNPWN associationassociation HESS J1825-137: Identification (mainly) by TeV spectral imaging > 2.5 TeV Aharonian et al. (HESS coll.) 1 – 1.52.5 TeV A&A 460, 2006 < 1 TeV AsymmetricAsymmetric VHEVHE PulsarPulsar WindWind NebulaeNebulae ''Crushed Plerions'' Offset VHE PWN Pulsar X-ray PWN VHE PWN Blondin et al., 2001 Or pulsar proper motion/ + IC electron lifetime larger than synchrotron lifetime + larger particle injection efficiency in the past ram pressure? ConfirmationConfirmation ofof thethe crushedcrushed PWNPWN scenarioscenario …… … in the HESS J1825-137 / G 18.0-0.7 system Pavlov et al., ApJ 675, 2008 pulsar proper motion (VLA) perpendicular to relic PWN direction HESSHESS J1813J1813--178:178: IdentificationIdentification withwith XX--rayray PWN?PWN? 2.5’ XMM-Newton Funk et al., A&A 470, 2007 If INTEGRAL source can be identified with X-ray (synchrotron) nebula → Object is a “Pevatron” HESSHESS J1813J1813--178:178: „„PevatronPevatron““ hypothesishypothesis Chandra: z Compact source: identified as pulsar z PWN dominates up to ~10 keV → INTEGRAL association Helfand et al., ApJ 665, 2007 with PWN not unplausible HESSHESS J1813J1813--178:178: IdentificationIdentification withwith XX--rayray PWN?PWN? INTEGRAL pulsars with known Edot Dean & Hill (astro-ph/0804.3420, RN): → Extreme pulsar properties z Either underluminous in INTEGRAL band (ε=0.01) z Or spin-down age decoupled from SNR age (cf. e.g. G11.2-0.3) HESSHESS J1809J1809--193:193: twotwo PSRPSR counterpartscounterparts Dean et al., MNRAS 384, 2008 + Chandra reanalysis INTEGRAL of G11.2-0.3 HESS J1809-193 (roughly) 50% of the 20-100 keV flux from PSR J1811- 1925 is from the PWN But no evidence for a morphological INTEGRAL 18-60 keV connection to the VHE source TheThe PWNPWN aroundaround PSRPSR J1809J1809--19171917 Chandra Chandra preliminary Kargaltsev & Pavlov, ApJ 670, 2007 HESS coll., Komin et al., astro-ph/0709.2432 HESS → The PWN around PSR J1809- 1917 is very likely contributing to HESS J1809-193 → Especially in this case, multiple components in the VHE source cannot be excluded preliminary VHEVHE PWNPWN candidatescandidates HESS coll., A&A 472, 2007 z Classification because of association with powerful pulsar z no X-ray PWN required for this classification z Large ε-values are in principle possible (decoupling from Edot) HESS coll., A&A 472, 2007 HESS collaboration, preliminary A&A, 2007 H.E.S.S. source of the month May 2007 HESS coll., Gallant
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